The sizes of the inner dust holes (r\(_{\rm in}\) ) for the HAeBes of our sample were estimated from their SEDs as follows. First, we assumed that the disk temperature decreases with the distance as T\(_{\rm disk}\)  = \(K\)  \(\times \)  r\(^{-3/4}\)  [1]}. For each star, the constant \(K\)  was estimated by replacing T\(_{\rm disk}\)  by the dust sublimation temperature T\(_{\rm sub}\) , assumed to be 2000 K, and \(r\)  by the dust sublimation radius, r\(_{\rm sub}\)  = R\(_*\) (T\(_{\rm sub}\) /T\(_*\) )\(^{-2.1}\)  [2]}. When the value of the constant is known, the size of the inner dust holes corresponding to the disk temperatures where the IR excess starts, determined from the Wien law and the SEDs, were derived from the above expression for T\(_{\rm disk}\) . The size of the inner dust holes is listed in Col. 8 of Table REF  along with its corresponding errors, which were determined by propagation considering the effective width of the photometric filter where the IR excess starts as the only uncertainty. As described in Sect. REF , the SED classification based on the JHK groups is directly related to the size of the inner disk dust holes estimated here, with the relative sizes increasing from group J to group \(>\)  K.
